The main selection function of the GALAH survey is relatively simple: it
avoids the crowded regions of the Galactic plane (\(|b|\)  > \(10^\circ \) ),
accounts for the nominal telescope operations (\(-80^\circ \le \delta \le +10^\circ \) ) and restricts observations by apparent magnitude (\(12 < V_{JK} <14\) ), while being colour independent. There is an additional requirement
for field selection: the density of stars has to be at least 400 per \(\pi \) 
square degrees to match the number of fibres and field of view of the fibre
positioner. The input catalogue for observations is based on the Two Micron
All-Sky Survey [1]}, with \(V_{JK}\) 
approximating standard \(V\)  magnitude and being computed as [2]}:
\(V_{JK} = K + 2(J-K + 0.14) + 0.382 \mathrm {e}^{(J-K - 0.2)/0.5}\) 
